2010
DOI: 10.1063/1.3495980
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Transport properties of high-temperature Jupiter atmosphere components

Abstract: Transport properties of high-temperature helium and hydrogen plasmas as well as Jupiter atmosphere have been calculated for equilibrium and nonequilibrium conditions using higher approximations of the Chapman–Enskog method. A complete database of transport cross sections for relevant interactions has been derived, including minority species, by using both ab initio and phenomenological potentials. Inelastic collision integrals terms, due to resonant charge-exchange channels, have been also considered.

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Cited by 70 publications
(53 citation statements)
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“…The bracket integrals, after some transformations, can be expressed in terms of collision integrals X ðk;rÞ cndm calculated for each pair of excited electronic states n and m of atoms c and d. In the present study we calculate the collision integrals using the models proposed in [24] but taking into account increasing atomic radius (i.e. effective cross-section) of electronically excited atoms.…”
Section: Transport Coefficientsmentioning
confidence: 99%
“…The bracket integrals, after some transformations, can be expressed in terms of collision integrals X ðk;rÞ cndm calculated for each pair of excited electronic states n and m of atoms c and d. In the present study we calculate the collision integrals using the models proposed in [24] but taking into account increasing atomic radius (i.e. effective cross-section) of electronically excited atoms.…”
Section: Transport Coefficientsmentioning
confidence: 99%
“…In the present study, the terms r = p = 0; r = 1, p = 0; r = 2, p = 0; and r = 0, p = 1 are retained [2]. The transport coe©cients are expressed in terms of the expansion coe©cients: 10 ;…”
Section: Transport Coefficientsmentioning
confidence: 99%
“…The integrals Ÿ (l,r) cd are calculated using the data from [10] for all types of collisions: neutral neutral, neutral charged, and charged charged interactions. For the transitions between electronic states, there is no accurate data on the relaxation times, which is necessary for calculating integrals β.…”
Section: Transport Coefficientsmentioning
confidence: 99%
“…In such cases, interfaces lead to strong concentration gradients and mixing. Many astrophysical situations also involve ionic transport in mixtures for the investigation of the composition of giant planets [8] and of the sedimentation of heavy elements in white dwarf stars [9], for instance.…”
Section: Introductionmentioning
confidence: 99%